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Constraining neutron star properties with a new equation of state insensitive approach

Dec 20, 2021

10 pages

Published in:

Phys.Rev.D 106 (2022) 4, 043012

Published: Aug 10, 2022

e-Print:

2112.10824 [astro-ph.HE]

DOI:

10.1103/PhysRevD.106.043012 (publication)

View in:

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Abstract: (APS)

Instead of parametrizing the pressure-density relation of a neutron star (NS), one can parametrize its macroscopic properties such as mass (

M

), radius (

R

), and dimensionless tidal deformability (

Λ

) to infer the equation of state (EOS) combining electromagnetic and gravitational wave (GW) observations. We present a new method to parametrize

R (M)

and

Λ (M)

relations, which approximates the candidate EOSs with accuracy better than 5% for all masses and spans a broad region of the

M - R - Λ

plane. Using this method we combine the

M - Λ

measurement from GW170817 and GW190425, and simultaneous

M - R

measurement of pulsars PSR

J 0030 + 0451

and PSR

J 0740 + 6620

to place joint constraints on NS properties. At 90% confidence, we infer

R_{1.4} = 12.0 5_{- 0.87}^{+ 0.98} km

and

Λ_{1.4} = 37 2_{- 150}^{+ 220}

for a

1.4 M_{⊙}

NS, and

R_{2.08} = 12.6 5_{- 1.46}^{+ 1.36} km

for a

2.08 M_{⊙}

NS. Furthermore, we use the inferred values of the maximum mass of a nonrotating NS

M_{\max} = 2.5 2_{- 0.29}^{+ 0.33} M_{⊙}

to investigate the nature of the secondary objects in three potential neutron star–black hole merger (NSBH) systems.

Note:

Published in PRD

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Figures(4)

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